Evolution of protoplanetary discs driven by the MRI, self-gravity and hydrodynamical turbulence

Details Evolution of protoplanetary discs driven by the MRI, self-gravity and hydrodynamical turbulence Evolution of protoplanetary discs driven by the MRI, self-gravity and hydrodynamical turbulence

Sep 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007mnras.380..311r&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 380, Issue 1, pp. 311-319.

Astronomy and Astrophysics

Astronomy

3

Accretion, Accretion Discs, Magnetic Fields, Mhd, Planetary Systems: Formation

Scientific paper

We study the viscous evolution of protoplanetary discs driven by the combined action of magnetohydrodynamic turbulence, resulting from the magneto-rotational instability (MRI), self-gravity torques, parametrized in terms of an effective viscosity and an additional viscous agent of unspecified origin. The distribution of torques driving the evolution of the disc is calculated by analysing where in the disc the MRI develops and, to incorporate the effect of self-gravity, calculating the Toomre parameter. We find that, generally, discs rapidly evolve towards a configuration where the intermediate regions, from a fraction of an au to a few au, are stable against the MRI due to their low-ionization degree. As an additional source of viscosity is assumed to operate in those regions, subsequent evolution of the disc is eruptive. Brief episodes of high mass accretion ensue as the criterion for the development of the MRI is met in the low-ionization region. The radial distribution of mass and temperature in the disc differs considerably from disc models with constant α parameter or layered accretion models, with potentially important consequences on the process of planet formation.

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